Revealing the coronal properties of Seyfert galaxies with NuSTAR Andrea Marinucci (Roma Tre) on behalf of the NuSTAR AGN Physics WG Dublin The X-ray Universe 2014 June 19, 2014
Overview Brief introduction on high-energy cutoff measurements Nearby AGN seen by NuSTAR Results Conclusions and future perspectives 1/20
Brief introduction on high-energy cutoff measurements Nearby AGN seen by NuSTAR Results Conclusions and future perspectives 2/20
Introduction One of the main open problem for AGN is the nature of the primary X-ray emission. It is due to Comptonization of soft photons, but the geometry, optical depth and temperature of the emitting corona are largely unknown. kt = 50 kev kt = 100 kev kt = 150 kev Most popular models imply Ecut=2-3x kte, so measuring Ecut helps constraining Comptonization models. 3/20
Introduction Since the primary X-ray radiation illuminates the disc and is partly reflected towards the observer's line of sight it is fundamental to properly take it into account. Variable PLC Constant RDC Fabian&Vaughan+03 Reynolds+96 4/20
Introduction So far, we have only a handful of results based on non focusing, and therefore strongly background-dominated, satellites (BeppoSAX-PDS, Suzaku HXD-PIN, INTEGRAL, Swift-BAT) Type 1 Type 2 Perola et al., 2002 De Rosa et al., 2012; Molina et al., 2013 5/20
Brief introduction on high-energy cutoff measurements Nearby AGN seen by NuSTAR Results Conclusions and future perspectives 6/20
The NuSTAR satellite 1 Ms Sensitivity Imaging 3.2 x 10-15 erg/cm2/s ( 6 10 kev) HPD 58 1.4 x 10-14 erg/cm2/s (10 30 kev) FWHM 18 Localization 2 (1-sigma) Spectral response energy range: 3-79 kev E @ 6 kev 0.4 kev FWHM E @ 60 kev 1.0 kev FWHM Harrison et al., 2013 Target of Opportunity response <24 hr typical 6-8 hours 80% sky accessibility 7/20
The NuSTAR satellite The combination of NuSTAR high effective area and low background yelds ~100x better S/N versus Suzaku HXD-PIN MCG-6-30-15: 125 ks net exposure time and same 15-70 kev flux (6.5x10-11 erg/cm2/s) Marinucci et al., 2014a 8/20
AGN observed by NuSTAR AGN Physics WG: Brenneman et al. 2014a Brenneman et al. 2014b Marinucci et al. 2014b Matt et al. 2014 9/20
Brief introduction on high-energy cutoff measurements Nearby AGN seen by NuSTAR Results Conclusions and future perspectives 10/20
NuSTAR cutoff measurements So far, NuSTAR has provided a number of cutoff measurements in AGN with different spectral characteristics: Relativistic reflection SWIFT J2127.4+5654 (Ec=108±10 kev), L2-10 kev=1.5x1043 erg/s Cold, distant reflection IC 4329A (Ec=186±14 kev), L2-10 kev=6.3x1043 erg/s Ark 120 (Ec>190 kev), L2-10 kev=5.6x1043 erg/s 11/20
Swift J2127.4+5654 NLS1 with a relativistically broadened Fe Kα emission line (a=0.6±0.2), a steep continuum (Γ=2-2.4), Ec=30-90 kev, Lbol/LEdd~0.18 (Miniutti+09, Malizia+08, Panessa+11, Sanfrutos+13) It was observed simultaneously with XMM-Newton for ~300 ks and both a strong Compton Hump and a broad Fe Kα line are present 13/20
Swift J2127.4+5654 When a model composed of a primary continuum, relativistic and distant reflection components is applied to the data the only residuals are above ~25 kev Marinucci et al. 2014b 12/20
Swift J2127.4+5654 When a model composed of a primary continuum, relativistic and distant reflection components is applied to the data the only residuals are above ~25 kev Marinucci et al. 2014b The inclusion of relxill model (Garcia & Dauser +14) allows us to measure a cutoff energy Ec=108±10 kev and to infer the contribution of the disk to the Compton hump. 12/20
Swift J2127.4+5654 Using comptt (Titarchuk+94) with two different geometries we get: SLAB kte=68+37-32 kev τ=0.35+0.35-0.19 SPHERE kte=53+28-26 kev τ=1.35+1.03-0.67 13/20
IC 4329A -Bright Sy1 galaxy, F2-10 kev ~ 0.1-1.8 x10-10 erg/cm2/s - Ec=100+200-40 kev (INTEGRAL+XMM, Molina+13) - Observed simultaneously by NuSTAR and Suzaku for ~120 ks in 2012 Brenneman et al. 2014b When a model composed of a primary continuum+reflection is applied to the data some residuals at high energies are found. 14/20
IC 4329A SPHERE SLAB No evidence for relativistic lines. Iron line and Compton reflection originate from distant material. 15/20
Ark 120 - Bare Seyfert 1 galaxy, F2-10 kev ~ 2-4 x10-11 erg/cm2/s - Prominent soft excess (XMM, Vaughan et al.+04) - Relativistic Iron line (Suzaku, Nardini et al.+11) - Observed simultaneously by NuSTAR and XMM for 90 ks in 2013 Vaughan et al. 2004 Nardini et al. 2011 16/20
Ark 120 When 0.5-80 kev data are considered the coronal parameters can be. derived, testing the optxagnf model (Done et al., 2012). The OM fluxes support an intermediate value for the black hole spin. 17/20
Brief introduction on high-energy cutoff measurements Nearby AGN seen by NuSTAR Results Conclusions and future perspectives 19/20
Conclusions High energy cut-off have been measured in a number of AGN with NuSTAR (more are yet to come!) The hard X-ray band (3-80 kev) is fundamental for testing and discriminating between different Comptonization models Further observations will help us in understanding the nature of the primary continuum, such as the relation between the accretion rate and the cutoff energy and the link between the disc reflection and the extension of the hot corona. 20/20